Extract green and red lines that we haven't got yet

Load up both cubes, as per previous notebooks.

Note that cube1 is the co-added data of various exposures, which has better s/n but slightly degraded angular resolution. This is the better choice for the weak lines.

Get all the regions from previous notebooks:

Start with the green range

So mcube is the one with better s/n, which we will generally be using.

Extract He I 5875 line

Fix sky as with Hβ

Make a wider window

Extract [Cl III] lines

Extract [N II] line

Second, the red range

The [Ar IV] auroral lines

Left to right

Also lots of sky lines

The [Cl IV] 7531 line

We can see a slight contamination by C II 7530.57, which comes from the filaments. But this is much better than before, now that I have reduced the wavelength range

The [Ar III] 7136 line

Need top fix the sky - use the standard method:

Make a wider window

Third, the far-red range

We just go as var as the Paschen limit, since there is no point fitting a polynomial across an ionization edge.

Look at the far red range for interesting bow shock lines

There is nothing much interesting in this range. Lots of weak He I lines. There are also a lot of low ionization lines, ssuch as Ca I], which I might want to come back to later.

This has the [Cl IV] 8045.62 line, although it is blended with a lower ionization line.

We can see a clear contamination by something coming from the filaments.

Fourth and finally, the infrared range

Those continuum fits are not very good, but nothing could fit those wobbles

Look at what we have got for the bow shock in the infrared range

Mostly H lines

The [S III] line and the brightest H line are all we need for the bow shock really. We could grab the [C I] line to though.

The [S III] 9069 line

Need top fix the sky - use the standard method:

Make a wider window